Prof. stavros katsanevas (university Paris 7/IN2P3/CNRS)
I will review the recently published roadmap of Astroparticle Physics by the AstroParticle Physics European Consortium (APPEC). I will in particular concentrate on the future challenges for European and Global Astroparticle Physics, with a special emphasis on the impact of the discovery of gravitational waves.
Michele Punturo (PG)
(Toward) the 3rd generation of GW observatories: Einstein Telescope
Dr Antoine PETITEAU (APC - Université Paris-Diderot)
The excellent results of the LISAPathfinder mission gave the green light for LISA mission. ESA approved the LISA mission as the large mission on the theme "The Gravitational Universe". This future observatory will observe gravitational wave from space between 0.02mHz and 1Hz, opening a new window on the Universe complementary to LIGO/Virgo and Pulsar Timing Array. The expected sources are...
Mr Jerome Degallaix (Laboratoire des Matériaux Avancés - CNRS)
Upgrade from second generation interferometers and third generation ones will require larger size optics as well as new material substrates to handle low temperatures. In parallel to this technological challenges, a worldwide intensive research is underway to lower the coating thermal noise from the mirrors. In this presentation, we will review the technological development and future plans...
Daniel Penkert (AEI Hannover)
The space-borne gravitational wave observatory LISA aims to measure sources in the 0.1 mHz to 1 Hz frequency range. Core to this measurement is the optical readout of differential path lengths between free-floating test masses aboard three satellites orbiting the sun in a tilted cartwheel formation. On average, the satellites’ positions form an equilateral triangle of 2.5 million km...
26. The Virgo Coating Collaboration: research lines and preliminary results of a detailed study on thermoelasticity in crystalline materials
Matteo Lorenzini (GSGC)
The visibility distance of interferometric gravitational wave detectors is limited by mirror thermal noise at mid-range frequency, where the first coalescence GW signals have been detected and where many others are expected in the next future. In particular, for 2G+ and 3G we need to increase the performance of the test mass multilayer reflective coatings. The Virgo collaboration is setting a...
16. The Virgo Coating Collaboration: a new deposition facility and preliminary results on nano-layered coatings
Dr Maria Principe (SA)
Thermal noise in the coatings of the test masses of the ground-based interferometric detectors of gravitational waves is the dominant noise contribution in the most sensitive frequency band, where the first gravitational signals have been detected and where several cosmic sources are deemed to exist. Hence developing coatings with reduced thermal noise is among the primary tasks of the Virgo...
Matteo Lorenzini (GSGC)
The performance of present and future gravitational wave detectors is limited by fundamental factors, such as thermal noise, seismic or newtonian noise and quantum nature of light. Besides, technological factors impact the reach of advanced detectors through status of art limits in the implementation of upgrade strategies. In the realm of optics, the quantum limit to sensitivity will be...
Dr Shtefan Danilishin (University of Glasgow)
It is hard to overestimate the scientific significance of the 6 confirmed detections of gravitational waves from compact binary sources that Advanced LIGO and Advanced Virgo have jointly made. However, it is still a long way ahead until the sensitivity of GW detectors is high enough to make them fully fledged astronomical tools. The main hindrance on this way remains the quantum noise, the...
Mrs Stefanie Kroker (PTB and TU Braunschweig)
Thermal noise is known to be a crucial limitation for high precision sensing devices like future gravitational wave detectors or lasers with extreme narrow linewidths. Mitigating Brownian thermal noise as an important issue requires the reduction of the mechanical loss of involved materials and/or their deliberate spatial distribution. In this contribution we discuss the influence of...
Dr Matteo Leonardi (NAOJ)
Kagra is the first 2.5G gravitational wave (GW) detector and it incorporates some very challenging new technologies such as underground facility and cryogenic sapphire mirrors. Another new technology that was not in the base road-map of any GW detector but nowadays is addressed as a crucial upgrade is frequency dependent squeezing. I'll give some highlights on the Kagra detector and...
Dr Antonio Perreca (TIFP)
The Laser Interferometer Gravitational-wave Observatory (LIGO) and Virgo have recently opened a new window for astronomy by detecting gravitational-waves from coalescing black holes and from neutron star merger. The LIGO/Virgo Scientific Collaboration is exploring ways to increase range and sensitivity by applying promising new techniques for current and next generation gravitational-wave...
6. Low temperature performances of a monolithic folded pendulum sensor for the third generation of interferometric detectors of gravitational waves
Flavio Travasso (PG)
An effective low frequency sensitivity improvement of the next generation of gravitational waves interferometric detectors requires the introduction of new ideas and the development of suitable technologies. Within this framework, the cryogenic suspensions represent a very good synthesis and effective approach to this problem, as already demonstrated by the KAGRA interferometric detector. An...
9. SAR-GRAV: the Sardinia Underground Laboratory, a first module for the Einstein Telescope infrastructure
Luca Naticchioni (ROMA1)
Since 2010 the site of Sos Enattos, a former mine in the North-East Sardinia - Italy, was studied with long term seismic investigations in the framework of the site selection for the Einstein Telescope (ET). The site proved to be one of the seismically quietest places in Europe, given the local geological features and the low population density of the island. In particular, in 2012 we realized...
31. Electromagnetic facilities and observing strategies for multimessenger science: situation and future perspectives.
In the advanced LIGO/Virgo era, a huge, world-wide effort have been put into the search of electromagnetic counteparts of gravitational wave (GW) events. Such effort has been carried out optimizing the use of the different observing facilities operating at all electromagnetic wavelengths and improving the data reduction and analysis procedures. This ultimately led to the hystorical detection...
Dr Antoine PETITEAU (APC - Université Paris-Diderot)
The LISA is an approved L3 ESA-NASA mission which aims at detecting gravitational wave signal in the milli-Hertz band. We are organizing set of LISA data challenges. The objectives of these challenges are 3-fold: (i) to release the data set which respects the latest changes in the LISA design and follows certain standards, this data will be open to anyone who wants to try their own data...
11. INTEGRAL observation of GW gamma ray counterparts and future perspectives: searching for Fermi/GBM un-triggered SGRB Candidates with INTEGRAL/PICsIT
James Rodi (INAF-IAPS)
The first detection of the prompt electromagnetic counterpart coincident with a GW170817 has been a forward step in our knowledge of NS-NS merging. An unexpected result was the extremely low isotropic luminosity of the event relative to other short gamma-ray bursts (SGRBs) with known redshifts, revealing a population of low luminosity SGRBs. The most popular interpretation has been that...
Dr Lorenzo Amati (INAF - IASF Bologna)
The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRBs and X-ray transients detection over a broad FOV...
Dr Aniello Grado (INAF-Osservatorio Astronomico di Capodimonte)
The discovery of the GW170817's optical counterpart has shown the wealth of information and science that can be gathered from such findings. As foreseen from theories and verified with the last GW event on the O2 run, the merging of two binary neutron stars produce a bright optical counterpart. The same is expected in the BH-NS coalescence while more controversial is the case of merging of...
Giovanni Andrea Prodi (TIFP)
Sebastiano Bernuzzi (PR)
Gravitational waves from neutron star collisions carry key information about matter at extreme densities. Advanced LIGO and Virgo can, for example, constrain the properties of zero-temperature neutron star's equation of state by estimating the tidal polarizability coefficients that parametrize the neutron stars' tidal interactions in the inspiral-merger phase. Third generation detectors might...
Albino Perego (MIB)
The first detection of GWs from a binary neutron star merger (GW170817) marked the beginning of the multimessenger astronomy era. A few hours after the GW detection, the observation of an associated electromagnetic counterpart compatible with a kilonova/macronova emission remarkably confirmed our basic picture concerning the ejection of matter and the nucleosynthesis occurring in such a kind...
Matteo Di Giovanni (TIFP)
The unprecedented observation of a binary neutron star coalescence by the Advanced Virgo and Advanced LIGO gravitational-wave detectors offers the opportunity to cast new light on neutron stars and matter under the most extreme conditions. Furthemore, for the first time we were able to observe the engine that powers events such as gamma ray bursts. After such a merger, a compact remnant is...
8. Recent results and future challenges for Continuous waves and Stochastic background searches with a network of gravitational wave detectors
Pia Astone (ROMA1)
Continuous gravitational waves and stochastic background searches are among the main targets of present and future gravitational wave searches. These sources have not been detected so far, anyhow important progresses have been made in the development of search procedures and significant constraints on source characteristics have, in some cases, been put. I will highlight the most recent...
Germano Nardini (University of Bern)
In this talk we review why the measurement of the stochastic gravitational wave background can shed light on the particle content of the Universe. We moreover sketch some popular particle physics theories for which LISA can prove the existence of new physics before colliders.
Prof. Emre Kahya (Istanbul Technical University)
The gravitational wave (GW) signal (GW170817) from the coalescence of binary neutron stars was simultaneously seen throughout the electromagnetic (EM) spectrum from radio waves to gamma-rays. We point out that this simultaneous detection rules out a class of modified gravity theories, and provides another indirect evidence for the existence dark matter.
Dr Sheng Yang (Observatory of Padova, INAF)
During the second science run(O2) of the Laser Interferometer gravitational-wave Observatory (LIGO) and Virgo Interferometer, a gravitational-wave signal consistent with a binary neutron star coalescence(BNS) was detected on 2017 August 17th (GW170817), quickly followed by a coincident short gamma-ray burst(GRB170817a) trigger by the Fermi satellite. 10 hours later, 6 groups independently...
38. MIGA and ELGAR : towards the observation of low frequency gravitational waves using atom interferometry
Dr Philippe BOUYER (CNRS - IOGS)
I will review the progress towards large-scale differential gravitational measurement is using an array of Atom Interferometers (AIs) configured to differentiate Newtonian Noise, geodetic signal and GW detection. In this gravitation antenna, each of the AIs measures the local gradient of gravitational acceleration and the correlation between distant sensors enables to cancel out fluctuations...
Mr Miguel Dovale-Alvarez (University of Birmingham)
Atom interferometers employing optical cavities to enhance the beam splitter pulses promise significant advances in science and technology, notably for future gravitational wave detectors. Long cavities, on the scale of hundreds of meters, have been proposed in experiments aiming to observe gravitational waves with frequencies below 1 Hz, where laser interferometers, such as LIGO, have poor...
Daniele Vetrugno (T)
The LIGO first detection officially opened the era of gravitational waves observation. Few weeks ago, the LISA Pathfinder team published its last results in which it was shown that the residual force noise between two test-masses in a single spacecraft can be reduced and measured at the level required by LISA, the Laser Interferometry Space Antenna. This result represents a milestone in...
29. The Free-fall Experiment Results: measuring subfemto-g acceleration noise in LISA Pathfinder and fN force variations on ground with torsion pendulum, in intermittent control mode
Giuliana Russano (Università di Trento/TIFPA)
The relative acceleration between two test masses free falling in orbit is perturbed by the presence of a larger constant relative acceleration that must be actively compensated in order to keep the test bodies centered inside the orbiting apparatus. The actuation force applied to compensate this effect can be applied continuously or can be limited to brief impulses, with test masses in a...
12. PETER: a torsion pendulum facility to study small forces/torques on free falling instrumented masses
Fabio Garufi (NA)
We will describe realization and tests of a two stage torsion pendulum facility (nicknamed PETER, from Italian PEndolo Traslazionale E Rotazionale, namely translational and Rotational Pendulum) for the measurement of GRS actuation Cross Talks (CT) and its possible evolution. This project started within the ground testing activities for the characterization, before flight, of the Gravitational...
Martina De Laurentis (NA)
One of the oldest questions concerning quantum mechanics and gravitation is whether vacuum fluctuations do gravitate. The question of the weight of vacuum was raised soon after the birth of quantum mechanics and many theoretical attempts were performed to explore the motivations and consequences of assuming or discarding such hypothesis, and jet today there no a complete theretical...
Dr Mario Spera (University of Innsbruck)
The first confirmation of the existence of merging stellar-mass black holes (BHs) came on September 14 2015, when the LIGO interferometers observed the gravitational-wave signal from the merger of two BHs with mass larger than 25 Msun (GW150914). Since then, four additional BH mergers were observed, and two of them have BHs with mass larger than 30 Msun. From the theoretical point of view,...
Nicola Giacobbo (University of Padova)
The recent detection of gravitational waves has proven the existence of massive stellar black hole binaries (BHBs), but the formation channels of BHBs are still an open question. Population-synthesis codes are one of the most powerful tools to investigate the origin of BHBs. In this talk, I describe my new code MOBSE, which is an updated version of the widely used binary population synthesis...
Marco Drago (TN)
Detections of stellar mass binary black holes (BBHs) system in the observing run of LIGO and VIRGO interferometers has started an exciting new era of black hole astrophysics. For understanding the formation channels of BBH a detected population of BBH will be required, with various parameters like masses, spins and orbital properties like eccentricity and precession. Hence, there is a strong...
Ms Elisa Bortolas (INAF-OAPd / University of Padova)
Super-massive black hole binaries (BHBs) are expected to be one of the most powerful sources of low-frequency gravitational waves (GWs) accessible to the forthcoming LISA mission. BHBs are believed to form in the late stages of galaxy mergers, then harden by close encounters with interacting stars, until GWs lead the BHBs to coalescence. In this talk, I will discuss how the encounter between a...
Giancarlo Cella (PI)
I review the scientific motivation to improve the sensitivity of earth bound interferometric detectors of gravitational waves in the low frequency region. I discuss the main issues and obstacles expected, with some possible solutions.